Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-54767
Fry, J N; Colombi, S; Fosalba, P; Balaraman, A; Szapudi, I; Teyssier, R (2011). Cell count moments in the halo model. Monthly Notices of the Royal Astronomical Society, 415(1):153-167.
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We study cell count moments up to fifth order of the distributions of haloes, of halo substructures as a proxy for galaxies, and of mass in the context of the halo model and compare theoretical predictions to the results of numerical simulations. On scales larger than the size of the largest cluster, we present a simple point cluster model in which results depend only on cluster-cluster correlations and on the distribution of the number of objects within a cluster, or cluster occupancy. The point cluster model leads to expressions for moments of galaxy counts in which the volume-averaged moments on large scales approach those of the halo distribution and on smaller scales exhibit hierarchical clustering with amplitudes Sk determined by moments of the occupancy distribution. In this limit, the halo model predictions are purely combinatoric, and have no dependence on halo profile, concentration parameter or potential asphericity. The full halo model introduces only two additional effects: on large scales, haloes of different mass have different clustering strengths, introducing relative bias parameters; and on the smallest scales, halo structure is resolved and details of the halo profile become important, introducing shape-dependent form factors. Because of differences between discrete and continuous statistics, the hierarchical amplitudes for galaxies and for mass behave differently on small scales even if galaxy number is exactly proportional to mass, a difference that is not necessarily well described in terms of bias.
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|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute for Computational Science|
|Deposited On:||18 Feb 2012 19:15|
|Last Modified:||31 Jan 2014 00:11|
|ISSN:||0035-8711 (P) 1365-2966 (E)|
|Additional Information:||The definitive version is available at www3.interscience.wiley.com|
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